A spectroscopic survey of thick disc stars outside the solar neighbourhood

In the previous sections we have shown how astronomical alignments and solar hierophanies – with a common interest in the solstices − were substantiated in the

As compared to high metallicity disc HII regions, CNSFR show values of the O 23 and the N2 parameters whose distributions are shifted to lower and higher values respectively,

Finally, experiments with solar [17–34], atmospheric [35–45], reactor [46–50], and long-baseline accelerator [51–59] neutrinos indicate that neutrino flavor change through

We find that the parameters of the model assumed for the radial profile of the rotational velocity, averaged over the considered lines of sight, are in agreement within two

In each panel, we show two MDFs derived from the simulations: one based upon the use of all star particles belonging to the bulge, after ap- plication of the kinematic

Second, the sample of less massive (M  ≤ 1.5 M  ) giant stars with planets covers the same mass range as the MS pro- genitors and subgiant stars where the metal signature has

The model with power-law density profile (Col. 4 in Table 6) gives the best overall fit to the SED, ISO-SWS spectrum and line emission (see Fig. 4), with quite different disc

As a means to probe the possible fractal structure of the galaxy distribution we have studied the scaling of the num- ber density and angular correlation function of galaxies